Hydrodynamical simulations of the barred spiral galaxy NGC 1365

Lindblad, P. A. B.; Lindblad, P. O.; Athanassoula, E.

doi:10.1007/bfb0101968

Cited by 30 publications

(41 citation statements)

References 6 publications

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“…The results of the two approaches may actually not have so many differences that the observations can distinguish. As already suggested by Lindblad & Lindblad (1994), it may be that the orbits out of this analytical model describe a gas flow similar to the one obtained with a hydrodynamic model. This hypothesis is supported by comparing the orbit pattern as shown in Fig.…”

Section: Discussionsupporting

confidence: 71%

“…The orbit patterns produced by this model exhibit some of the main features expected in barred potentials, e.g., the elongated orbits, the phase shift change at an ILR, and the spiral pattern. Also, they match observations and results of numerical simulations (see Lindblad & Lindblad 1994). This analytical approach should be particularly suitable for NGC 4569 which, as noted in Sect.…”

Section: Descriptionsupporting

confidence: 77%

“…Comparisons of the two approaches are discussed in Lindblad & Lindblad (1994), Wada (1994), and Regan et al (1999). The analytical model of orbits in a barred potential presented in the previous section effectively traces the evolution of gas particles in the gravitational potential as they are subjected to collisions.…”

Section: Discussionmentioning

confidence: 99%

“…This model was introduced and developed by Sanders & Huntley (1975), Lindblad & Lindblad (1994), Wada (1994), OFFSET Sakamoto et al (1999) and Baker (2000). It is based on analytical solutions for the orbits of gas particles obtained by a perturbation calculation of the epicyclic stellar motions.…”

Section: Descriptionmentioning

confidence: 99%

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Molecular gas in NUclei of GAlaxies (NUGA)

Boone

Baker

Schinnerer

et al. 2007

A&A

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Section: Discussionsupporting

confidence: 71%

Section: Descriptionsupporting

confidence: 77%

Section: Discussionmentioning

confidence: 99%

Section: Descriptionmentioning

confidence: 99%

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Molecular gas in NUclei of GAlaxies (NUGA)

Boone

Baker

Schinnerer

et al. 2007

A&A

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“…NGC 2366 (Wevers et al 1986) has a regular bi-symmetric velocity field. For NGC 1313, the Ha-data from Marcelin & Athanassoula (1982) indicated the possibility of an offset bar, but the Hi-data from Peters et al (1988) and the new AT data from Ryder et al (1994) show otherwise.…”

Section: Sbm -Ibm Galaxiesmentioning

confidence: 97%

Global Rotational Properties of Barred Galaxies

Bosma¹

1996

International Astronomical Union Colloquium

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Detailed comparison of the structures and kinematics of simulated and observed barred galaxies

O'Neill

Dubinski

2003

Monthly Notices of the Royal Astronomical Society

102

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We examine the observable properties of simulated barred galaxies, including radial mass profiles, edge‐on structure and kinematics, bar lengths and pattern speed evolution for detailed comparison to real systems. We have run several simulations in which bars are created through inherent instabilities in self‐consistent simulations of a realistic disc+halo galaxy model with a disc‐dominated, flat rotation curve. These simulations were run at high (N= 20 million particles) and low (N= 500 000 particles) resolution to test numerical convergence. We determine the pattern speeds in simulations directly from the phase angle of the bar versus time and the Tremaine–Weinberg method. Fundamental dynamics do not change between the high and low resolution, suggesting that convergence has been reached in this case. We find that the higher resolution is needed to simulate structural and kinematic properties accurately. The edge‐on view of the higher‐resolution system shows the bending instability and formation of a peanut‐shaped bulge clearly. We determined bar lengths by different means to determine that the simulated bar is fast, with a corotation to bar length ratio of under 1.5. Simulated bars in these models form with pattern speeds slower than those observed and slow‐down during their evolution. Dynamical friction between the bar and dark halo is responsible for this deceleration, as revealed by the transfer of angular momentum between the disc and the halo. However, even though the pattern speed is reduced at later times, the instantaneous scalelength of the disc has grown sufficiently for the bar motion to agree with many observations. By using a different model and simulation technique than other authors, we are able to compare the robustness of these methods. An animation of the face‐on and edge‐on views of the 20‐million‐particle simulation is available at http://www.astro.utoronto.ca/~oneill.

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Hydrodynamical simulations of the barred spiral galaxy NGC 1365

Cited by 30 publications

References 6 publications

Molecular gas in NUclei of GAlaxies (NUGA)

Molecular gas in NUclei of GAlaxies (NUGA)

Global Rotational Properties of Barred Galaxies

Detailed comparison of the structures and kinematics of simulated and observed barred galaxies

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